A Study of the Coronal Plasma in RS CVn binary systems: HR 1099 and co
Abstract
XMM-Newton has been performing comprehensive studies of X-ray luminous RS CVn binary systems in its calibration and guaranteed time programs. We present results from ongoing investigations in the context of a systematic study of coronal emission from RS CVns. We concentrate here on coronal abundances and investigate the abundance pattern in RS CVn binaries as a function of activity and average temperature. We find a transition from an Inverse First Ionization Potential (FIP) effect towards an absence of a clear trend (no FIP) in intermediately active RS CVn systems. This scheme fits well into the long-term evolution from an IFIP to a FIP effect found in solar analogs. We further study variations in the elemental abundances during a large flare.
Cite
@article{arxiv.astro-ph/0109264,
title = {A Study of the Coronal Plasma in RS CVn binary systems: HR 1099 and co},
author = {M. Audard and M. Guedel and A. Sres and R. Mewe and A. J. J. Raassen and E. Behar and C. R. Foley and R. L. J. van der Meer},
journal= {arXiv preprint arXiv:astro-ph/0109264},
year = {2007}
}
Comments
to appear in 35th ESLAB Symposium "Stellar Coronae in the Chandra and XMM-Newton Era", eds. F. Favata & J.J. Drake (San Francisco: ASP), in press